Title: Dynamical Stability of Terrestrial and Giant Planets in the HD 155358 Planetary System
Abstract:The results of a study of the dynamical evolution and the habitability of the planetary system of HD 155358 are presented. This system is unique in that it is one of the two low metallicity stars disc...The results of a study of the dynamical evolution and the habitability of the planetary system of HD 155358 are presented. This system is unique in that it is one of the two low metallicity stars discovered to host a multiple planet system. HD 155358 is host to two Jupiter-sized planets, with minimum masses of 0.86 and 0.50 Jupiter-masses. The orbit of the lower mass planet of this system is located at the inner edge of the system's habitable zone. To determine whether this system can harbor terrestrial-type planets, the orbits of its planets and an Earth-like object were numerically integrated for different values of their masses and orbital eccentricities. Results indicate that this system could potentially host stable orbits for terrestrial-sized planets in its habitable zone, but the stability of these orbits is very sensitive to the precise characteristics of the giant planets of the system. The long-term stability of larger bodies (Neptuneand Saturn-mass) was also studied in this system. Results show that a Neptuneor Saturn-mass body could exist in stable orbits in this system fairly close in, potentially within the range of present detection techniques, again depending on the precise configurations of the giant planets.Read More
Publication Year: 2007
Publication Date: 2007-10-01
Language: en
Type: article
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Title: $Dynamical Stability of Terrestrial and Giant Planets in the HD 155358 Planetary System
Abstract: The results of a study of the dynamical evolution and the habitability of the planetary system of HD 155358 are presented. This system is unique in that it is one of the two low metallicity stars discovered to host a multiple planet system. HD 155358 is host to two Jupiter-sized planets, with minimum masses of 0.86 and 0.50 Jupiter-masses. The orbit of the lower mass planet of this system is located at the inner edge of the system's habitable zone. To determine whether this system can harbor terrestrial-type planets, the orbits of its planets and an Earth-like object were numerically integrated for different values of their masses and orbital eccentricities. Results indicate that this system could potentially host stable orbits for terrestrial-sized planets in its habitable zone, but the stability of these orbits is very sensitive to the precise characteristics of the giant planets of the system. The long-term stability of larger bodies (Neptuneand Saturn-mass) was also studied in this system. Results show that a Neptuneor Saturn-mass body could exist in stable orbits in this system fairly close in, potentially within the range of present detection techniques, again depending on the precise configurations of the giant planets.